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The jets in a microquasar are modelled using a three-dimensional relativistic hydrocode (PLUTO), with the aim of investigating the appearance of equatorial radio emission. A dynamical mechanism is explored whereby the bow shocks of the jets strongly affect the equatorial regions. The presence of an extended disc is assumed and its role proves to be important in producing equatorial emission. As a concrete example, we focus on the SS 433 microquasar, one of the most intensively studied objects in the Galaxy, for which equatorial emission has been repeatedly detected during the last decade.

The jets in a microquasar are modelled using a three-dimensional relativistic hydrocode (PLUTO), with the aim of investigating the appearance of equatorial radio emission. A dynamical mechanism is explored whereby the bow shocks of the jets strongly affect the equatorial regions. The presence of an extended disc is assumed and its role proves to be important in producing equatorial emission. As a concrete example, we focus on the SS 433 microquasar, one of the most intensively studied objects in the Galaxy, for which equatorial emission has been repeatedly detected during the last decade.